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We present numerical simulations of terrestrial planet formation that examinethe growth continuously from planetesimals to planets in the inner SolarSystem. Previous studies show that the growth will be inside-out, but it isstill common practice to assume that the entire inner disk will eventuallyreach a bi-modal distribution of embryos and planetesimals. For thecombinations of disk mass, initial planetesimal radius and gas disk lifetimeexplored in this work the entire disk never reaches a simple bi-modal massdistribution. We find that the inside-out growth is amplified by the combinedeffects of collisional evolution of solid bodies and interactions with adissipating gas disk. This leads to oligarchic growth never being achieved indifferent places of the disk at the same time, where in some cases the disk cansimultaneoulsy support chaotic growth and giant impacts inside 1 au and runawaygrowth beyond 2 au. The planetesimal population is efficiently depleted in theinner disk where embryo growth primarily advances in the presence of asignificant gas disk. Further out in the disk growth is slower relative to thegas disk dissipation, resulting in more excited planetesimals at the same stageof growth and less efficient accretion. This same effect drives mass loss dueto collisional grinding strongly altering the surface density of the accretedplanets relative to the initial mass distribution. This effect decreases theMars-to-Earth mass ratios compared to previous works with no collisionalgrinding. Similar to some previous findings utilizing vastly different growthscenarios these simulations produce a first generation of planetary embryosthat are stable for 10-20 Myr, or 5-10 e-folding times of the gas dissipationtimescale, before having an instability and entering the chaotic growth stage.

Planetesimals to Terrestrial Planets: collisional evolution amidst a dissipating gas disk